The gentle monster PDS 456 - Kiloparsec-scale molecular outflow and its implications for QSO feedback

We report on the first ALMA observation of the CO(3？2) and rest-frame ～340 GHz continuum emission in PDS 456, which is the most luminous, radio-quiet QSO in the local Universe (z？？？0.18), with a bolometric luminosity L_{Bol？～？10^{47 erg s？1. ALMA angular resolution allowed us to map scales as small as ～700 pc. The molecular gas reservoir traced by the core of the very bright CO(3？2) emission line is distributed in a compact rotating disk, with a size of ～1.3 kpc, seen close to face-on (i？～？25 deg). Fast CO(3？2) emission in the velocity range v？∈？[？？？1000,？500] km s？1 is also present. Specifically, we detect several blue-shifted clumps out to ～5 kpc from the nucleus, in addition to a compact (R？？？1.2 kpc), broad emission component. These components reveal a galaxy-wide molecular outflow, with a total mass (for an αCO？=？0.8？M⊙ (K km s？1 pc2)？1) and a mass outflow rate ？mol ～ 290 M⊙ yr？1. The corresponding depletion time is τdep？～？8 Myr, shorter than the rate at which the molecular gas is converted into stars, indicating that the detected outflow is potentially able to quench star-formation in the host. The momentum flux of the molecular outflow normalised to the radiative momentum output (i.e. LBol/c) is ？1, comparable to that of the X-ray ultra-fast outflow (UFO) detected in PDS 456. This is at odds with the expectations for an energy-conserving expansion suggested for most of the large-scale outflows detected in low-luminosity AGNs so far. We suggest three possible scenarios that may explain this observation: (i) in very luminous AGNs such as our target the molecular gas phase is tracing only a fraction of the total outflowing mass; (ii) a small coupling between the shocked gas by the UFO and the host-galaxy interstellar medium (ISM); and (iii) AGN radiation pressure may be playing an important role in driving the outflow}}